The magnetosphere of Uranus at solstice (the time of the Voyager 2 flyby). Upper left and right panels show the configuration at different phases of the planet’s 18-hour spin period (see Bagenal, Ann. Rev. Earth Planet. Sci., 20, 289, 1992). The lower panel shows a numerical simulation of the helical magnetotail (Toth et al., JGR, 109, A11210, 2004).
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The magnetosphere of Neptune in the configuration corresponding tothe time of the Voyager 2 fly-by (see Bagenal, Ann. Rev. Earth Planet. Sci., 20, 289, 1992). Over the 19-hour spin period the magnetospheric plasma sheet in the tail changes from roughly planar to cylindrical.
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The draping of tubes of solar magnetic flux around a conducting ionosphere such as that of Venus. The flux tubes are slowed down and sink into the wake to form a tail (after Saunders and Russell 1986).
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Interaction of the solar wind with the atmosphere, ionosphere, and magnetized crust of Mars. The several processes whereby the planet may have lost much of its atmosphere are shown.
Credit: Fran Bagenal & Steve Bartlett
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